Although these objections may appear daunting, there is good reason to believe the validity of the RVM in many cases. In PSR J1906+0746 where the geometry changes with time due to precession of the beam, the RVM tracks the geometrical changes beautifully [1]}. Furthermore, in pulsars with interpulses, RVM fitting reflects the geometry of both the main and interpulse components [2]}, [3]}. In this paper we therefore attempt RVM fits for a sample of more than 1200 pulsars observed using the MeerKAT telescope. Section 2 briefly outlines the observations and the calibration procedure. Section 3 describes how the RVM fitting was performed and Section 4 details the results of the fitting. In Section 5 we present an analysis of the results and their implications for the population of pulsars as a whole.
<FIGURE><FIGURE><FIGURE>